M33（HERM33ES）中致密250 μm发射区和HII区的性质
Properties of compact 250 μm emission and HII regions in M33 (HERM33ES)
摘要：
在HERM33ES重点项目的框架内，利用Herschel测光数据的高分辨率和高灵敏度，我们研究了本星系群旋涡星系M33的致密发射，以探讨致密SPIRE发射源的性质。我们提取了250微米的源目录，以调查这种紧凑的排放的性质。利用这些波长前所未有的赫歇尔分辨率，我们还专注于对银河系北部一些引人注目的Halalpha壳进行更精确的研究。我们提出了一个目录中的159个紧凑的发射源在M33中确定的SExtractor在250微米SPIRE波段，这是一个提供最佳的空间分辨率。我们还测量了这些159个提取的源在24 μ m和Halpha的通量。贝壳的形态学研究也受益于多波长方法，包括Halpha，GALEX的远紫外线以及Spitzer IRAC 8um和MIPS 24um的红外线，以便进行比较。对于在250 μ m处选择的159个紧凑源，我们发现与MIPS 24 μ m发射的Pearson相关系数非常强（r24 = 0.94），与H α发射的相关性相当强，尽管具有更多的散射（rHa = 0.83）。的形态学研究的Halpha壳显示远紫外线，Halpha，和SPIRE带之间的位移。SPIRE的冷尘埃发射清楚地描绘了Halalpha壳层结构。通过从HII区域的标准配方中恢复恒星形成率，250 μ m紧凑型发射与24 μ m和Halpha发射之间的非常强的联系使我们能够仅基于250 μ m紧凑型发射提供恒星形成率校准。相对于SPIRE冷尘埃辐射的不同位置的Halalpha和远紫外辐射导致Halalpha壳层和相关冷尘埃的动力学年龄为几百万年。
英文摘要：
Within the framework of the HERM33ES Key Project, using the high resolution and sensitivity of the Herschel photometric data, we study the compact emission in the Local Group spiral galaxy M33 to investigate the nature of the compact SPIRE emission sources. We extracted a catalogue of sources at 250um in order to investigate the nature of this compact emission. Taking advantage of the unprecedented Herschel resolution at these wavelengths, we also focus on a more precise study of some striking Halpha shells in the northern part of the galaxy. We present a catalogue of 159 compact emission sources in M33 identified by SExtractor in the 250um SPIRE band that is the one that provides the best spatial resolution. We also measured fluxes at 24um and Halpha for those 159 extracted sources. The morphological study of the shells also benefits from a multiwavelength approach including Halpha, far-UV from GALEX, and infrared from both Spitzer IRAC 8um and MIPS 24um in order to make comparisons. For the 159 compact sources selected at 250um, we find a very strong Pearson correlation coefficient with the MIPS 24um emission (r24 = 0.94) and a rather strong correlation with the Halpha emission, although with more scatter (rHa = 0.83). The morphological study of the Halpha shells shows a displacement between far-ultraviolet, Halpha, and the SPIRE bands. The cool dust emission from SPIRE clearly delineates the Halpha shell structures. The very strong link between the 250um compact emission and the 24um and Halpha emissions, by recovering the star formation rate from standard recipes for HII regions, allows us to provide star formation rate calibrations based on the 250um compact emission alone. The different locations of the Halpha and far-ultraviolet emissions with respect to the SPIRE cool dust emission leads to a dynamical age of a few Myr for the Halpha shells and the associated cool dust.
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